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Space Weather: Terrestrial Perspective 太空天气:地球视角
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2007-05-23 DOI: 10.12942/lrsp-2007-1
Tuija Pulkkinen
{"title":"Space Weather: Terrestrial Perspective","authors":"Tuija Pulkkinen","doi":"10.12942/lrsp-2007-1","DOIUrl":"https://doi.org/10.12942/lrsp-2007-1","url":null,"abstract":"<p>Space weather effects arise from the dynamic conditions in the Earth’s space environment driven by processes on the Sun. While some effects are influenced neither by the properties of nor the processes within the Earth’s magnetosphere, others are critically dependent on the interaction of the impinging solar wind with the terrestrial magnetic field and plasma environment. As the utilization of space has become part of our everyday lives, and as our lives have become increasingly dependent on technological systems vulnerable to space weather influences, understanding and predicting hazards posed by the active solar events has grown in importance. This review introduces key dynamic processes within the magnetosphere and discusses their relationship to space weather hazards.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2007-05-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2007-1","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5219261","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 242
Kinetic Physics of the Solar Corona and Solar Wind 日冕和太阳风的运动物理
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2006-07-27 DOI: 10.12942/lrsp-2006-1
Eckart Marsch
{"title":"Kinetic Physics of the Solar Corona and Solar Wind","authors":"Eckart Marsch","doi":"10.12942/lrsp-2006-1","DOIUrl":"https://doi.org/10.12942/lrsp-2006-1","url":null,"abstract":"<p>Kinetic plasma physics of the solar corona and solar wind are reviewed with emphasis on the theoretical understanding of the <i>in situ</i> measurements of solar wind particles and waves, as well as on the remote-sensing observations of the solar corona made by means of ultraviolet spectroscopy and imaging. In order to explain coronal and interplanetary heating, the micro-physics of the dissipation of various forms of mechanical, electric and magnetic energy at small scales (e.g., contained in plasma waves, turbulences or non-uniform flows) must be addressed. We therefore scrutinise the basic assumptions underlying the classical transport theory and the related collisional heating rates, and also describe alternatives associated with wave-particle interactions. We elucidate the kinetic aspects of heating the solar corona and interplanetary plasma through Landau- and cyclotron-resonant damping of plasma waves, and analyse in detail wave absorption and micro instabilities. Important aspects (virtues and limitations) of fluid models, either single- and multi-species or magnetohydrodynamic and multi-moment models, for coronal heating and solar wind acceleration are critically discussed. Also, kinetic model results which were recently obtained by numerically solving the Vlasov-Boltzmann equation in a coronal funnel and hole are presented. Promising areas and perspectives for future research are outlined finally.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2006-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2006-1","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5039395","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 578
Topological Methods for the Analysis of Solar Magnetic Fields 分析太阳磁场的拓扑方法
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2005-12-01 DOI: 10.12942/lrsp-2005-7
Dana W. Longcope
{"title":"Topological Methods for the Analysis of Solar Magnetic Fields","authors":"Dana W. Longcope","doi":"10.12942/lrsp-2005-7","DOIUrl":"https://doi.org/10.12942/lrsp-2005-7","url":null,"abstract":"<p>The solar coronal magnetic field is anchored to a complex distribution of photospheric flux consisting of sunspots and magnetic elements. Coronal activity such as flares, eruptions and general heating is often attributed to the manner in which the coronal field responds to photospheric motions. A number of powerful techniques have been developed to characterize the response of the coronal field by describing its <i>topology</i>. According to such analyses, activity will be concentrated around topological features in the coronal field such as separatrices, null points or bald patches. Such topological properties are insensitive to the detailed geometry of the magnetic field and thereby create an analytic tool powerful and robust enough to be useful on complex observations with limited resolution. This article reviews those topological techniques, their developments and applications to observations.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2005-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-7","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4010867","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 178
Starspots: A Key to the Stellar Dynamo 星斑:恒星发电机的钥匙
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2005-12-01 DOI: 10.12942/lrsp-2005-8
Svetlana V. Berdyugina
{"title":"Starspots: A Key to the Stellar Dynamo","authors":"Svetlana V. Berdyugina","doi":"10.12942/lrsp-2005-8","DOIUrl":"https://doi.org/10.12942/lrsp-2005-8","url":null,"abstract":"<p>Magnetic activity similar to that of the Sun is observed on a variety of cool stars with external convection envelopes. Stellar rotation coupled with convective motions generate strong magnetic fields in the stellar interior and produce a multitude of magnetic phenomena including starspots in the photosphere, chromospheric plages, coronal loops, UV, X-ray, and radio emission and flares. Here I review the phenomenon of starspots on different types of cool stars, observational tools and diagnostic techniques for studying starspots as well as starspot properties including their temperatures, areas, magnetic field strengths, lifetimes, active latitudes and longitudes, etc. Evolution of starspots on various time scales allows us to investigate stellar differential rotation, activity cycles, and global magnetic fields. Together these constitute the basis for our understanding of stellar and solar dynamos and provide valuable constraints for theoretical models.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2005-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-8","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4010271","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 352
Surface Evolution of the Sun’s Magnetic Field: A Historical Review of the Flux-Transport Mechanism 太阳磁场的表面演化:通量输运机制的历史回顾
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2005-10-18 DOI: 10.12942/lrsp-2005-5
Neil R. Sheeley Jr.
{"title":"Surface Evolution of the Sun’s Magnetic Field: A Historical Review of the Flux-Transport Mechanism","authors":"Neil R. Sheeley Jr.","doi":"10.12942/lrsp-2005-5","DOIUrl":"https://doi.org/10.12942/lrsp-2005-5","url":null,"abstract":"<p>This paper reviews our attempts to understand the transport of magnetic flux on the Sun from the Babcock and Leighton models to the recent revisions that are being used to simulate the field over many sunspot cycles. In these models, the flux originates in sunspot groups and spreads outward on the surface via supergranular diffusion; the expanding patterns become sheared by differential rotation, and the remnants are carried poleward by meridional flow. The net result of all of the flux eruptions during a sunspot cycle is to replace the initial polar fields with new fields of opposite polarity. A central issue in this process is the role of meridional flow, whose relatively low speed is near the limit of detection with Doppler techniques. A compelling feature of Leighton’s original model was that it reversed the polar fields without the need for meridional flow. Now, we think that meridional flow is central to the reversal and to the dynamo itself.</p><p>An upcoming <i>Living Reviews</i> article by Marc DeRosa on the more technical details and consequences of the model will supplement this historical review.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2005-10-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-5","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4735079","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 89
The Solar Wind as a Turbulence Laboratory 太阳风作为湍流实验室
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2005-09-20 DOI: 10.12942/lrsp-2005-4
Roberto Bruno, Vincenzo Carbone
{"title":"The Solar Wind as a Turbulence Laboratory","authors":"Roberto Bruno,&nbsp;Vincenzo Carbone","doi":"10.12942/lrsp-2005-4","DOIUrl":"https://doi.org/10.12942/lrsp-2005-4","url":null,"abstract":"<p>In this review we will focus on a topic of fundamental importance for both plasma physics and astrophysics, namely the occurrence of large-amplitude low-frequency fluctuations of the fields that describe the plasma state. This subject will be treated within the context of the expanding solar wind and the most meaningful advances in this research field will be reported emphasizing the results obtained in the past decade or so. As a matter of fact, Ulysses’ high latitude observations and new numerical approaches to the problem, based on the dynamics of complex systems, brought new important insights which helped to better understand how turbulent fluctuations behave in the solar wind. In particular, numerical simulations within the realm of magnetohydrodynamic (MHD) turbulence theory unraveled what kind of physical mechanisms are at the basis of turbulence generation and energy transfer across the spectral domain of the fluctuations. In other words, the advances reached in these past years in the investigation of solar wind turbulence now offer a rather complete picture of the phenomenological aspect of the problem to be tentatively presented in a rather organic way.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2005-09-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-4","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4805264","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 117
Dynamo Models of the Solar Cycle 太阳周期的发电机模型
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2005-06-13 DOI: 10.12942/lrsp-2005-2
Paul Charbonneau
{"title":"Dynamo Models of the Solar Cycle","authors":"Paul Charbonneau","doi":"10.12942/lrsp-2005-2","DOIUrl":"https://doi.org/10.12942/lrsp-2005-2","url":null,"abstract":"<p>This paper reviews recent advances and current debates in modeling the solar cycle as a hydromagnetic dynamo process. Emphasis is placed on (relatively) simple dynamo models that are nonetheless detailed enough to be comparable to solar cycle observations. After a brief overview of the dynamo problem and of key observational constraints, we begin by reviewing the various magnetic field regeneration mechanisms that have been proposed in the solar context. We move on to a presentation and critical discussion of extant solar cycle models based on these mechanisms. We then turn to the origin of fluctuations in these models, including amplitude and parity modulation, chaotic behavior, and intermittency. The paper concludes with a discussion of our current state of ignorance regarding various key questions, the most pressing perhaps being the identification of the physical mechanism(s) responsible for the generation of the Sun’s poloidal magnetic field component.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2005-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-2","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4538728","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 41
Coronal Waves and Oscillations 日冕波和振荡
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2005-05-07 DOI: 10.12942/lrsp-2005-3
Valery M. Nakariakov, Erwin Verwichte
{"title":"Coronal Waves and Oscillations","authors":"Valery M. Nakariakov,&nbsp;Erwin Verwichte","doi":"10.12942/lrsp-2005-3","DOIUrl":"https://doi.org/10.12942/lrsp-2005-3","url":null,"abstract":"<p>Wave and oscillatory activity of the solar corona is confidently observed with modern imaging and spectral instruments in the visible light, EUV, X-ray and radio bands, and interpreted in terms of magnetohydrodynamic (MHD) wave theory. The review reflects the current trends in the observational study of coronal waves and oscillations (standing kink, sausage and longitudinal modes, propagating slow waves and fast wave trains, the search for torsional waves), theoretical modelling of interaction of MHD waves with plasma structures, and implementation of the theoretical results for the mode identification. Also the use of MHD waves for remote diagnostics of coronal plasma — MHD coronal seismology — is discussed and the applicability of this method for the estimation of coronal magnetic field, transport coefficients, fine structuring and heating function is demonstrated.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2005-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-3","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4630938","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Magnetic Fields in the Solar Convection Zone 太阳对流区的磁场
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2004-12-01 DOI: 10.12942/lrsp-2004-1
Yuhong Fan
{"title":"Magnetic Fields in the Solar Convection Zone","authors":"Yuhong Fan","doi":"10.12942/lrsp-2004-1","DOIUrl":"https://doi.org/10.12942/lrsp-2004-1","url":null,"abstract":"<p>Recent studies of the dynamic evolution of magnetic flux tubes in the solar convection zone are reviewed with focus on emerging flux tubes responsible for the formation of solar active regions. The current prevailing picture is that active regions on the solar surface originate from strong toroidal magnetic fields generated by the solar dynamo mechanism at the thin tachocline layer at the base of the solar convection zone. Thus the magnetic fields need to traverse the entire convection zone before they reach the photosphere to form the observed solar active regions. This review discusses results with regard to the following major topics:\u0000</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2004-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2004-1","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4009924","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 152
Astrospheres and Solar-like Stellar Winds 天体球和类太阳恒星风
IF 20.9 1区 物理与天体物理
Living Reviews in Solar Physics Pub Date : 2004-07-29 DOI: 10.12942/lrsp-2004-2
Brian E. Wood
{"title":"Astrospheres and Solar-like Stellar Winds","authors":"Brian E. Wood","doi":"10.12942/lrsp-2004-2","DOIUrl":"https://doi.org/10.12942/lrsp-2004-2","url":null,"abstract":"<p>Stellar analogs for the solar wind have proven to be frustratingly difficult to detect directly. However, these stellar winds can be studied indirectly by observing the interaction regions carved out by the collisions between these winds and the interstellar medium (ISM). These interaction regions are called “astrospheres”, analogous to the “heliosphere” surrounding the Sun. The heliosphere and astrospheres contain a population of hydrogen heated by charge exchange processes that can produce enough H I Ly<i>α</i> absorption to be detectable in UV spectra of nearby stars from the <i>Hubble Space Telescope</i> (HST). The amount of astrospheric absorption is a diagnostic for the strength of the stellar wind, so these observations have provided the first measurements of solar-like stellar winds. Results from these stellar wind studies and their implications for our understanding of the solar wind are reviewed here. Of particular interest are results concerning the past history of the solar wind and its impact on planetary atmospheres.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2004-07-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2004-2","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5115571","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 97
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